Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-10T21:54:16.935Z Has data issue: false hasContentIssue false
  • English
  • Français

Tidal barrier and the asymptotic mass of proto gas-giant planets

Published online by Cambridge University Press:  01 October 2007

Ian Dobbs-Dixon ,
ShuLin Li  and
Douglas N.C. Lin
Ian Dobbs-Dixon
Affiliation:
Department of Physics, McGill University, Montreal, Canada email: iandd@physics.mcgill.ca
ShuLin Li
Affiliation:
Department of Astronomy, Peking University, Beijing, China email: m.lugaro@phys.uu.nl
Douglas N.C. Lin
Affiliation:
Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA email: lin@ucolick.org
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Although late stage gap formation reduces the surface density in the vicinity of protoplanets, simulations suggest gas may continue to leak through the protoplanets tidal barrier, replenishing the gas supply and allowing protoplanets to acquire masses comparable to or larger than that of Jupiter. Global gas depletion is a possible explanation for gaseous planets with lower masses in weak-line T-Tauri disks and ice giants in our own solar system, but it is unlikely to have stalled the growth of multiple systems around nearby stars that contain relatively low-mass, close-in planets along with more massive and longer period companions. Here, we suggest a potential solution. We show that supersonic infall of surrounding gas onto a protoplanet is only possible interior to both its Bondi and Roche radii. Although the initial Bondi radius is much smaller than its Roche radius, the former overtakes the latter during its growth. Thereafter, a positive pressure gradient is required to induce the gas to enter the Roche lobe of the protoplanet and flow is significantly reduced. We present the results of analysis and numerical simulations to show that the accretion rate increases rapidly with the ratio of the protoplanets Roche to Bondi radii. Based on these results we suggest that in regions with low geometric aspect ratios gas accretion is quenched, resulting in relatively low protoplanetary masses.

Keywords

planet formationaccretion
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 263 - 266
Copyright
Copyright © International Astronomical Union 2008

References

D'Angelo, G., Henning, T., & Kley, W. 2002, A&A, 385, 647Google Scholar
Garaud, P. & Lin, D. N. C. 2007, ApJ, 654, 606Google Scholar
Goldreich, P. & Tremaine, S. 1979, ApJ, 233, 857CrossRefGoogle Scholar
Goldreich, P. & Tremaine, S. 1980, ApJ, 241, 425CrossRefGoogle Scholar
Haisch, K. E. Jr., Lada, E. A., & Lada, C. J. 2001, ApJL, 553, L153CrossRefGoogle Scholar
Ida, S. & Lin, D. N. C. 2004, ApJ, 604, 388CrossRefGoogle Scholar
Kley, W., D'Angelo, G., & Henning, T. 2001, ApJ, 547, 457CrossRefGoogle Scholar
Korycansky, D. G. & Papaloizou, J. C. B. 1996, ApJS, 105, 181CrossRefGoogle Scholar
Lin, D. N. C. & Papaloizou, J. 1979, MNRAS, 186, 799Google Scholar
Lin, D. N. C. & Papaloizou, J. 1985, in Protostars and Planets II, ed. Black, D. C. & Matthews, M. S., 981–1072Google Scholar
Lin, D. N. C. & Papaloizou, J. 1986, ApJ, 309, 846CrossRefGoogle Scholar
Lubow, S. H., Seibert, M., & Artymowicz, P. 1999, ApJ, 526, 1001CrossRefGoogle Scholar
Marcy, G., Butler, R. P., Fischer, D., Vogt, S., Wright, J. T., Tinney, C. G., & Jones, H. R. A. 2005, Progress of Theoretical Physics Supplement, 158, 24Google Scholar
Papaloizou, J. C. B. & Terquem, C. 2006, Reports of Progress in Physics, 69, 119CrossRefGoogle Scholar
Tanigawa, T. & Watanabe, S.-i. 2002, ApJ, 580, 506CrossRefGoogle Scholar